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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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LARGEST OPTICAL TELESCOPES
Cre
dits: E
SO
Doubling diameter time = 28yrs
The key technology: active optics
1989 ESO NTT 3.6m
Cre
dits: E
SO
/C.M
adse
n Subaru 8.2m primary mirror
Jump
4m 8m
The key technologies:
• primary segmentation
• adaptive optics
Jump 8m 30m
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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ADAPTIVE OPTICS CONCEPT AND TIMELINE
Credits: C. Max
1953 Babcock: the concept
70s US Military: first real system
1989 first AO astronomical system, COME-ON
1997 NAOS@VLT (185acts)
2000 Keck NGS
2000 Gemini North
2003 MACAO@VLT
2006 NAOS + Na Laser
2007 MAD@VLT (experiment)
2010-12 LBT FLAO 1&2 and LBTI
2012 GEMS @Gemini South
2014 GPI@ Gemini S. (already on the mountain)
2014 SPHERE@VLT (ongoing acceptance test Europe)
2015 AOF@VLT
2020-.... ELTs: adaptive telescopes
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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Simard
H-band
Seeing limited Vs. AO corrected
H-band
The first high contrast image
2 AO systems commissioned 2010-2012
THE FIRST HIGH CONTRAST AO SYSTEM Large Binocular Telescope, the new generation of AO
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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Exo
planets
HR8799 first H-band
detection of 4 planets.
Constrain on the planet
atmoshperic model.
Esposito et al. 2013
Skemer et al. 2012
IR data combined with
radio ones are
consistent with outflow
and disk structures
Cesaroni al. 2013
Star
formation
THE FIRST HIGH CONTRAST AO SYSTEM Large Binocular Telescope, the new generation of AO
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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Position accuracy 0.5mas
Proper motion detectd
0.3mas/yr
Close et al. 2012
Globular cluster age
can be estimated
considering the
difference of the
two knees (red)
Bono et al.
in submission
Theta Ori trapezium
20
arc
sec
HST/WFC3 F110W
integration = 21 min. LBT AO Ks-band
Integration = 10 min.
LBT no AO J - K
(wide field) FLAO+PISCES J -
K
(narrow field)
HST H - FLAO+P. K
(narrow field field)
?
Astrometry
Crowded fields
THE FIRST HIGH CONTRAST AO SYSTEM Large Binocular Telescope, the new generation of AO
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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HIGH CONTRAST,
23M INTERFEROMETER READY TO GO
Simard
HOSTS Hunt for Observable Signatures of Terrestrial planetary Systems
The first survey to detect faint warm dust from collisions in asteroid
belts around other stars. Detection of the dust would indicate a
planetary system similar to ours, with small rocky bodies.
LEECH LBTI Exozodi, Exoplanet Common Hunt
Parallel observations of the same stars during the HOSTS survey at
4 microns wavelength. These observations will be sensitive to
Jupiter-like gas giant planets.
Ro
be
rge
et a
l. 2
01
2
Zodiacal dust around other stars can obscure flux from an exo-Earth.
At 10 times our own density (10 zodies) the dust will impact the
performance of exo-Earth imaging missions.
LBTI is designed to probe for zodiacal dust at 10 µm down to 10
zodies. It is unique in being able to accomplish this task
NASA-supported 60 night survey to be
carried out in the 2013-2016 time frame.
Top level goal is to reduce risk for future
NASA exoplanet imaging missions
0.25s @10.6 µm
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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MAIN AO SYSTEM TYPES
Natural Guide Star
Single Conjugated
Requires a bright star I<15 @20’’
Scientific field d ~ 40’’ diameter in K
Na Laser Guide Star
Single Conjugated
Requires a faint star I<17 @1’
Scientific field d ~ 40’’ diameter in K
Multi Conjugated
Requires multiple faint star I<17 @1’
Scientific field d ~ 1.5’ diameter in K
... and many more
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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Simard
THE FIRST LASER MCAO SYSTEM
GeMS performance is very uniform over a 85x85 arcsec square field,
both in terms of Strehl ratios and more general PSF characteristics;
Sky coverage of ~55% for all the portion of the sky reachable from
Gemini South
1.5 to 1.7 magnitude sensitivity gain over the 1-2.5 micron range on
point sources with respect to seeing limited imaging.
Gains with respect to HST/NICMOS, in the same conditions, are 0.3 (J)
and 1.2 (K) magnitudes;
Asterims of 5 Na Laser Guide
Stars arrenged on a square
2 deformable mirrors 5 Shack-Hartmann
Wavefront Sensors
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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3.0 arcmin
3.9
arc
min
Seeing @550nm
0.6-1.1arcsec
H2 – Fe II – Ks
FWHM 90mas
Cre
dit: G
em
ini O
bse
rvato
ry / A
UR
A
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
Ideal resolution for knots and filament study
1pix = 7AU
[HST Helix program resolution28AU]
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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Seeing limited @Ks
FWHM = 0.9arcsec
Integration = 19.4min
Brandl et al. 2005
Antennae Galaxies
GeMS AO 2012
FWHM = 0.1arcsec
Integration = 8min
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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sensitivity gain with AO
for ELT is 10 times more than 8m
Cre
dits: G
MT
Scie
nce
bo
ok
AO GAIN ON 30M TELESCOPES
5s detection limits in 1h of integration @1mm gain of factor 30 (Seeing 0.5’’)
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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Giant Magellan Telescope www.gmto.org
Diameter 24m 30m 39m
Segments 7 X 8.4m 492 X 1.44m 798 x 1.45m
Collecting area 368m2 660m2 1077m2
Diffraction limit @1mm 9mas 7mas 5mas
AO Systems SCAO, LTAO, GLAO
(6 Na Lasers)
SCAO, MCAO
(6 Na LGS)
SCAO, GLAO, LTAO, MOAO,
MCAO, XAO (6 Na Lasers)
First Science 2020 4 segments only
(2022 full)
2022 2023
Cost 700 M$ 1000 M$
1000 M€
Thirty Meter Telescope www.tmt.org
European - ELT www.eso.org/public/teles-instr/e-elt
THE EXTREMELY LARGE TELESCOPES
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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ELT’S SCIENCE CASES
• Cosmology & fundamental physics
• Early Universe
• Galaxy formation and evolution
• Black holes
• Stellar population and chemical evolution
• Extra solar planetary systems
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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GIANT MAGELLAN TELESCOPE
Adaptive secondary mirror
feeding all the focal stations
7 deformable shells of 1.1m
4700 actuators
SCAO
LTAO
GLAO
High spatial
resolution instruments
Wide field
instruments
Aplanatic Gregorian
No Nasmyth focus
Primary f/0.7
Gregorian focus f/8
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
Instrument / Mode Capabilities λ Range, μm Resolution Field of View
G-CLEF / NS, GLAO Optical High Resolution
Spectrometer / PRV 0.35 – 0.95 20 – 100K
7 x 0.7,1.2”
fibers
GMTIFS / LTAO, NGSAO NIR IFU / Imager 0.9 – 2.5 5,000 & 10,000 10 / 400 arcsec2
GMACS / NS, GLAO Wide-Field Optical Multi-Object
Spectrometer 0.36 – 1.0
1,500 – 4,000
(10K with MANIFEST) 40-60 arcmin2
GMTNIRS / NGSAO, LTAO JHKLM High Resolution
Spectrometer 1.2 – 5.0 50K, 100K 1.2” long-slit
MANIFEST* / NS, GLAO Facility Robotic Fiber Feed 0.36 – 1.0 20’ diameter
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THE INSTRUMENT SUITE
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dits: G
. Ja
co
by
[20
19-2
02
1]
Spectral resolution Angular resolution
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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INSTRUMENT SUITE
Classic Ritchey-Chrétien configuration
Postfocal AO system providing:
MCAO
SCAO
LTAO
(GLAO)
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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EUROPEAN ELT
Instruments - First Light
AO Mode λ (µm) Resolution FoV / Sampling Add. Mode
E-CAM – 2023
SCAO, MCAO
- IMG - MRS
0.8 – 2.4 BB, NB 3000
53.0” / 3 mas Astrometry 40mas Coronography
E-IFU – 2023
SCAO, LTAO
- IFU 0.5 – 2.4 4000 10 000 20 000
0.5×1.0” / 4mas 5.0×10.0” / 40mas
Coronography
E-MIDIR – 2024/2028
SCAO, LTAO
- IMG - MRS - IFU
3 – 13 3 - 13 3 - 5
BB, NB 5000 100 000
18” / 12 mas 0.4”×1.5” / 4 mas
Coronography Polarimetry
E-HIRES - 2024/2028
SCAO
- HRS
0.37 – 0.71 0.84 – 2.50
200 000 120 000
0.82” 0.027”×0.5”
Polarimetry
E-MOS - 2024/2028
MOAO
Slits IFUs IFUs
0.37 – 1.4 0.37 – 1.4 0.8 – 2.45
300- 2500 5000 – 30 000 4000 – 10 000
6.8” / 0.1” 420’ / 0.3” 2” / 40mas
Multiplex ~ 400 Multiplex ~100 Multiplex ~10 Imaging?
E-PCS - 2027/2030
XAO EPOL IFS
0.6 – 0.9 0.95 – 1.65
125 – 20 000
2.0” / 2.3 mas 0.8“ / 1.5 mas
Coronography Polarimetry
1st light
2nd light
SCAO
GLAO
LTAO
MCAO
MOAO
XAO
5 mirror optical design
M4: a 2.5 adaptive mirror w/ 4800 actuators
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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DYNAMICS OF HIGH REDSHIFT GALAXIES
Simulated ELT-IFU observation of Ha
Ima
ge
s: H
AR
MO
NI co
nso
rtiu
m
(sim
ula
tio
ns b
y T
im G
oo
dsa
ll)
• shocks, winds, interaction with IGM
• dynamical masses
• rotation (kinematics),
• chemical composition (fraction of
heavy metals) • Major or minor mergers?
• Are rotating disks present?
• Accretion of hot or cold gas?
ULIRG at z~2
Mergers at z~4
Puech et al 2008
Simulated major merger z = 4 (1.4bn yrs)
ELT-IFU + MOAO
75mas/pix 150x150mas2
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
E-ELT provides resolution to probe sphere of influence
• 106M BH at Virgo distance
• 109M BHs to z~0.2
Image credit: NASA/Dana
Berry, SkyWorks Digital
SUPERMASSIVE BLACK HOLES
Ve
locity d
ispe
rsio
n
Ve
locity
1.25e7 M⊙ BH no BH
3 ”
Resolution 50mas (SINFONI@VLT) 0.8 ”
1.25e7 M⊙ BH no BH
Ve
locity d
isp
ers
ion
V
elo
city
• Statistical samples
• Understand scatter in MBH-s relation
Resolution 5mas (E-ELT + LTAO)
Test case: simulation of NGC4486 at 16Mpc (Virgo)
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SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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Natural seeing 0.6’’
Simulated
K-band imaging of a dense star cluster
HST - NICMOS
JWST NIRCAM
GMT Strehl Ratio 80%
CROWDED FIELDS
Credit: P. McCarthy
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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CROWDED FIELDS
Central 30arcsec of M32 in the NIR
Gemini AO (2000) JWST TMT AO
Credit: TMT Science Book
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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PROTO PLANETARY DISK
E-MIDIR simulations of high-contrast
imaging at 10 µm
• Jupiter footprint at 20 AU (@100pc) from G-star
• Gap detection at a few mJy/as2
at 0.1-0.2” (10 – 20 AU)
• ELT-MIR very competitive with JWST
Credits: G. Chauvin
Asymmetry Asymmetry
and spyral
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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EXO-PLANETS DIRECT IMAGING
Credits: TMT Science Book
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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GIANT EXOPLANET ATMOSPHERES
• Reflected, Transmitted or Emitted light of Exoplanets
• Strongly or non-strongly irradiated planets
• Physics of Planetary Atmospheres (Giant, Exo-Neptunes to Super-Earths)
- Geometric Albedos
- Chemical Composition
(H20, CH4, CO, CO2, NH3…)
- Atmosphere’s Dynamics
. Inversion
. Vertical Mixing
. Circulation
. Evaporation
Knutson et al. 09
Spitzer
No Thermal Inversion Thermal inversion
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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EXO-EARTH IN THE HZ DETECTION (RV)
Expected planet population detected by Doppler spectroscopy with: o HARPS on the ESO 3.6-metre (precision 1 ms−1; left), o ESPRESSO on the VLT(precision 10 cms−1; middle) o and CODEX on the E-ELT(precision 1 cms−1; right)
CODEX, required to detect Earth-like planets in Habitable Zone of solar-type stars
Credits: G. Chauvin
HARPS (ESO 3.6m) ESPRESSO (VLT) CODEX (E-ELT)
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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SYNERGIES The «questions»:
• Are there habitable planets around near stars?
• How and when did the first stars begin to shine?
• Can we model the complex physics that is involved in the formation of
stars, galaxies, and supermassive black-holes?
• … and much more
The answer will come from the synergy between: • Big radio telescope arrays (ALMA, ...)
• Next generation of space telescopes (JWST,...)
• ELTs
• Next generation of ground based survey telescopes (LSST, ...)
• New generation of solar telescopes (EST)
Spectral line sensitivity Angular resolution
SIF XCIX Congresso Nazionale – Trieste, 26 Settembre 2013
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• The key technology for the ELTs is Adaptive Optics
• The current forefront AO systems for 8m telescopes are:
• the FLAO system of LBT (INAF) for the high contrast
• GeMS at Gemini South as the first multi conjugated laser
system
• 3 ELTs upcoming in the next decade
• All will implement several AO systems to exploit their huge
apertures in angular resolution and sensitivity
• The ELT’s instruments will span l from 0.35 to 20mm with R
up to 200k to explore from the solar system to the first light
objects
• ELTs will create a strong synergy with new generation of
satellites and radio arrays
CONCLUSIONS